The number of orbits used exceeds the number allocated The specified Bright Earth Avoidance angle is outside the permitted range. FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser The specified Bright Earth Avoidance angle is outside the permitted range. FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser The specified Bright Earth Avoidance angle is outside the permitted range. The specified Bright Earth Avoidance angle is outside the permitted range. Unschedulable Visit The specified Bright Earth Avoidance angle is outside the permitted range. FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser Unschedulable Visit The specified Bright Earth Avoidance angle is outside the permitted range. Submitted with substantial changes to Visit01: Epoch 01 of 13 is a 4-orbit (pseudo)CVZ visit, using the opportunity at ORIENT = 081.9 degrees. After guide star acquisition at the start of the first orbit, the guide star remains visible and locked for the duration of the visit, so no guide star re-acquisition in subsequent orbits will be required in orbits 2--4. This strategy is the same as adopted for GO-15278 in Cycle 25, and as successfully executed through Cycle 27. An additional pre-pattern exposure has been added for OBAD follow-on needs. Custom targeting (modulated by small dither POSTARGs) has been implemented for this visit, because of severe guidestar paucity at the intended location within the 13-epoch pattern. While APT throws an error for the specified Bright Earth Avoidance angle of 13.5 degrees, this value is intended and proven to schedule for a pseudo-CVZ visit. 04/27/2021 - ROYLE - Submitting an update to visits 05 and 08 on behalf of PI 06/04/2021 - ROYLE - Submitting an update to visit 06 on behalf of PI. Changes to FLASH values. -------- 07/15/2021 - GROGIN - 1st submission of the continuation program 16793 (from 16252), for guidestar checking 10/05/2021 - ROYLE - Updates to 16793 visit 01 (modified from previous pointing and added leading exposure) 04/21/2022 - JANSEN - raised natural background observed in past 3 visits allows reducing post-flash by 1 e- for the longer WFC3/UVIS F275W exposures and still meet the minimum background of 20 e- /pix. -807812950 ----- Attempting Submission 4 (Tue Jun 30 23:39:07 GMT 2020) ----- ----- Attempting Submission 5 (Thu Aug 13 17:09:53 GMT 2020) ----- ----- Attempting Submission 6 (Thu Sep 03 20:11:32 GMT 2020) ----- ----- Attempting Submission 7 (Fri Oct 16 15:58:24 GMT 2020) ----- ----- Attempting Submission 8 (Wed Nov 04 15:55:35 GMT 2020) ----- ----- Attempting Submission 9 (Fri Mar 12 13:28:41 GMT 2021) ----- ----- Attempting Submission 10 (Tue Apr 27 16:19:40 GMT 2021) ----- ----- Attempting Submission 11 (Fri Jun 04 13:42:13 GMT 2021) ----- ----- Attempting Submission 12 (Fri Jul 16 03:36:55 GMT 2021) ----- ----- Attempting Submission 13 (Tue Oct 05 15:28:19 GMT 2021) ----- ----- Attempting Submission 14 (Thu Apr 21 20:54:52 GMT 2022) ----- Minor modification of requested post-flash only per consult with our PC Patricia Royle. We propose to complete the near-contiguous UV-Visible imaging of the JWST NEP Time-Domain Field, the best field within the JWST Continuous Viewing Zones to conduct deep and wide extragalactic JWST surveys at arbitrary cadence or orientation. This recently developed, ~14' diameter time-domain field near the North Ecliptic Pole (1) is devoid of sources brighter than m_AB ~ 16 mag at 2-4 micron that would deeply saturate JWST/NIRCam, (2) has the lowest possible zodiacal foreground, (3) has low Galactic foreground extinction, and (4) has a wealth of deep ground- and space-based ancillary data from X-ray through radio. Deep UV-Visible HST imaging to m_AB ~ 28 mag exists for the inner ~9' diameter portion of this field. Completing the coverage of the NEP Time-Domain Field to the same depth, in combination with extant data, allows the community to: (1) Establish a baseline UV-Visible detection image at ~0.07" FWHM at wavelengths inaccessible to JWST, and map transients and moving objects in areas of 2- and 3-epoch overlap; (2) Identify rest-frame UV-bright objects at z < 6 that would contaminate JWST ultra-high-z galaxy samples; (3) Identify galaxies with steep intrinsic UV-Visible SEDs indicative of (weak)AGN, assess the escape of LyC photons at 2 < z < 3, and place limits on that escape and IGM porosity at z < ~3.5; and (4) Study mass assembly and evolution of all significantly resolved UV-bright galaxies at z < 6 on a 'pixel-by- pixel' basis. In order to maximize the scientific return of early-release JWST science, it is critical to image this field in the UV-Visible while HST is still in its prime and before commencement of JWST observations in 2022. This treasury program was allocated 28 primary plus 28 parallel orbits in Cycle 28, and 24 primary plus 24 parallel orbits in Cycle 29, and aims to complete near-contiguous 3-filter UV--visible HST imaging of the JWST North Ecliptic Pole (NEP) Time-Domain Field, for which allocated GTO observations will provide both NIRCam 8-band imaging and NIRISS slitless spectroscopy at four distinct "spokes". JWST ERS and GO observers will have access to the GTO data, so we anticipate time-domain follow-up as early as JWST Cycle 1, as well as additional areal coverage within this field. The JWST NEP Time-Domain Field was defined to be the cleanest ~14' diameter area in JWST's northern Continuous Viewing Zone (CVZ), where JWST can conduct a deep extragalactic time-domain survey, with added utility for extreme outer solar system and near-Galactic time-domain science. The present program, GO-16252+GO-16793, builds directly on Cycle 25 program GO-15278, which covered the inner ~5' diameter portion of the field, by imaging an annulus surrounding the extant observations to very similar depths. We aim to minimize both gaps between new and extant data, and overlap with those extant data, while maximizing use of (pseudo)CVZ opportunities in Cycle 28 and 29. To maximize (1) overall HST coverage of the JWST NEP Time-Domain Field, (2) overlap of the UV coverage of WFC3/UVIS F275W and visible coverage of ACS/WFC F435W and F606W, and (3) execute this program as efficiently as possible, we specify seven (Cycle 28) + six (Cycle 29) 4-orbit visits using (pseudo)CVZ orbits with orientations and POS TARG offsets such that WFC3/UVIS F275W observations at one orientation will largely overlap ACS/WFC F435W and F606W obervations at an alteranate orientation in our overall pattern. This observational design brings our program to the total of 52 primary and 52 coordinated parallel orbits approved in Phase I. Through experimentation in Cycle 25 Phase II, we found that the visits optimize better when we define the ACS/WFC observations as primary and the WFC3/UVIS observations as coordinated parallels. This does not change the intent or scope of this program. The final detailed layout takes into account the availability of suitable guide stars for each visit, which forced a slight offset of ~30" of visit #1 with respect to the ideal pointing. While we designed the detailed observations for the full Cycle 28+29 program, this Phase-II APT of GO-16793 covers only Cycle 29, i.e., the final 6 out of 13 visits. We are a team of junior, post-doctoral, mid-career, and senior scientists that represent the talent and expertise needed to perform the proposed analyses of the HST data, and interpret these on their own and in concert with ancillary data within the JWST NEP Time-Domain Field. Briefly: Dr. Rolf Jansen (PI) has over 19 years of experience analyzing HST data from FOC, STIS, WFPC2, ACS, and WFC3. As Co-I of JWST GTO program #1176, he serves as team lead for the JWST NEP Time-Domain Field (e.g., Jansen &amp; Windhorst 2018), and is PI of Cycle 25 program GO15278. He is also PI of the LBT/LBC Ugriz imaging of the JWST NEP Time-Domain Field and its surroundings. He has mentored undergraduates (e.g., via the ASU/NASA Space Grant program), and (co-)advised graduate students at ASU resulting in published dissertation papers using HST data, ranging from resolved stellar populations within local dwarfs, through clues to mass-assembly from the shapes of radial surface brightness profiles of galaxies at z=4--6, to high-z quasar hosts, and LyC escape. Dr. Norman Grogin is an expert at the design and implementation of challenging, large observing programs with HST, including (UV)CANDELS and GO15278. His interests include normal galaxies and AGN hosts. Dr. Rogier Windhorst is an Interdisciplinary Scientist for JWST, and is the PI of GTO program #1176, which will image the 14' diameter JWST NEP TDF with NIRCam at 0.8--5 micron (~47 hrs). His interests include LyC escape from galaxies and AGN, and caustic crossings of First Light sources. Dr. Anton Koekemoer is expert on HST image combination and mosaicing techniques for large, complex programs, and will produce the HST mosaics for the JWST NEP TDF. His science interests include high-z galaxies and AGN. Dr. Christopher Willmer is a JWST/NIRCam team member and PI of MMT/MMIRS near-IR imaging, and MMT/Binospec+MMIRS spectroscopy. Dr. Seth Cohen (HST image analysis; PI of IRAM30m/Nika2 mm observations) Dr. Chris Conselice (galaxy evolution, morphology, lensing, spectroscopy; PhD mentor of Mr. Alex Griffiths). Dr. Mehmet Alpaslan (galaxy clustering and mass assembly). Dr. Matthew Ashby (PI of Spitzer/IRAC proposals; mid-IR properties of galaxies). Dr. Teresa Ashcraft (LBT/LBC near-UV imaging and data analysis). Drs. Silvia Bonoli and Renato Dupke (narrow-band spectrophotometry; PIs of J-PAS spectrophotometric observations). Dr. Walter Brisken (PI of high-resolution, multi-phase center VLBA radio observations). Dr. Francesca Civano (PI of NuSTARR hard X-ray proposal). Drs. Bill Cotton and Rick Perley (scheduling, reduction, and interpretation of VLA data). Dr. Vik Dhillon (optical time-domain science; PI of GTC/HiPERCAM imaging). Dr. Simon Driver (extragalactic background light, galaxy populations). Drs. Ken Duncan and Huub Rottgering (LOFAR long-wave radio, and WEAVE spectroscopy). Dr. Martin Elvis (high-energy transients science). Dr. Giovanni Fazio (PI of the Spitzer/IRAC instrument, PI of SMA sub-mm interferometry). Dr. Steven Finkelstein (ultra-high-z universe and galaxy evolution; PhD mentor of Ms. Rebecca Larson). Dr. Brenda Frye (gravitational lensing related transients; PI of LBT AO near-IR spectroscopy). Dr. Heidi Hammel (JWST IDS and PI of GTO program #1255; solar system science). Dr. Nimish Hathi (galaxy mass-assembly, and HST specialist). Ms. Minhee Hyun (sub-mm galaxies). Ms. Victoria Jones (astrometry, variable sources in HST/LBT/Subaru data; senior thesis mentored by the PI). Mr. Duho Kim (galaxy SEDs, extinction by dust; Ph.D. candidate with the PI and Dr. Windhorst). Dr. Bilal Ladjelate (mm-wave science, observations and analysis). Dr. W. Peter Maksym (high-energy transients; PI of Chandra X-ray monitoring programs). Dr. Sangeeta Malhotra (high-z emission-line objects, epoch of reionizaton, grism spectroscopy). Ms. Madeline Marshall (high-z AGNs, reionization and galaxy formation simulations). Dr. Hugo Messias (AGN demographics; X-ray through sub-mm). Dr. Stefanie Milam (extreme solar system objects). Dr. James Rhoads (GRB and high-z transients science; epoch of reionization; PI of WFIRST grism SIT). Dr. Steve Rodney (high-z SN science; Ph.D. mentor of Mr. Justin Roberts-Pierel). Dr. Michael Rutkowski (early-type galaxies, UV dust extinction, and LyC escape). Dr. Russell Ryan (Galactic stars and sub-stellar objects; grism spectroscopy). Drs. Ian Smail and Myungshin Im (dusty galaxies; PIs of JCMT/Scuba2 sub-mm imaging). Dr. Brent Smith (high-z LyC escape from AGN and galaxies, IGM transmission). Drs. Martin Ward and Nico Cappelluti (co-PIs of XMM-Newton 0.3-10keV X-ray monitoring proposal). Dr. Reinout van Weeren (large-scale structure formation, long-wave radio and X-ray). Mr. Cameron White (high-z AGN candidates, photometry, SEDs; senior thesis mentored by the PI). 6 false false false false false false false AVAILABLE UNIDENTIFIED HIGH LATITUDE FIELD INFRARED EMITTER OPTICAL EMITTER ULTRAVIOLET EMITTER The target field is centered on the extant HST observations of the JWST NEP Time-Domain Field of GO-15278. Allocated JWST GTO observations will provide both NIRCam imaging and NIRISS slitless spectroscopy in this field, which was defined to be the cleanest ~14' diameter area in JWST's northern continuous viewing zone, where JWST will conduct a deep extragalactic time-domain survey, with added utility for extreme outer solar system and near-Galactic time-domain science. The JWST NEP Time-Domain Field is developed as a *community field*, and has deep coverage accross the electromagnetic spectrum from X-ray through long-wave radio. The present Cycle 28+29 HST program will complete near-contiguous 3-filter coverage in the UV--Visible, targeting the annulus surrounding the extant HST observations of GO-15278. The present Phase-II APT specifies the Cycle 29 pointings within that annulus. J2000 1638381062884 5714 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/royle/OP-cache/16793-v01.xml Copy of Epoch 08 of 13 is a 4-orbit (pseudo)CVZ visit, using the opportunity at alternative ORIENT = 061.75 degrees. After guide star acquisition at the start of the first orbit, the guide star remains visible and locked for the duration of the visit, so no guide star re-acquisition in subsequent orbits will be required in orbits 2--4. This strategy is the same as adopted for GO-15278 in Cycle 25, and as successfully executed through Cycle 28. Specified POS_TARGs with respect to the nominal field center place the instrument apertures at the intended location within the 13-epoch pattern. While APT throws an error for the specified Bright Earth Avoidance angle of 13.5 degrees, this value is intended, and proven to schedule and execute successfully for a pseudo-CVZ visit. 1634351283000 61.18000000000009 (Tic-Visit :proposal-id 16793 :visit-id "01" :proposal-version -1 :trans-version "20210514" :date "01-Dec-2021 12:51:02.0" :trans-errors '(:WARNINGS 21 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 13.5 :data-volume 7430512 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16793 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16793 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 5332 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "01" :orbit-number 2 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "01" :orbit-number 3 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "01" :orbit-number 4 :pcs-time 0 :si-vis-utilization 5522 :al-overhead-at-end 0 :internal-dur-at-end 193 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "01" :orbit-number 5 :pcs-time 0 :si-vis-utilization 0 :al-overhead-at-end 0 :internal-dur-at-end 506 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) true 5 3 The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. 1638381626073 5714 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/royle/OP-cache/16793-v02.xml Epoch 09 of 13 is a 4-orbit (pseudo)CVZ visit, using the opportunity at ORIENT = 003 degrees. After guide star acquisition at the start of the first orbit, the guide star remains visible and locked for the duration of the visit, so no guide star re-acquisition in subsequent orbits will be required in orbits 2--4. This strategy is the same as adopted for GO-15278 in Cycle 25, and as successfully executed through Cycle 28. Specified POS_TARGs with respect to the nominal field center place the instrument apertures at the intended location within the 13-epoch pattern. While APT throws an error for the specified Bright Earth Avoidance angle of 13.5 degrees, this value is intended, and proven to schedule and execute successfully for a pseudo-CVZ visit. 1639086468000 3.0 (Tic-Visit :proposal-id 16793 :visit-id "02" :proposal-version -1 :trans-version "20210514" :date "01-Dec-2021 13:00:25.0" :trans-errors '(:WARNINGS 22 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 13.5 :data-volume 7430512 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16793 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16793 :visit-id "02" :orbit-number 1 :pcs-time 383 :si-vis-utilization 5332 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "02" :orbit-number 2 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "02" :orbit-number 3 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "02" :orbit-number 4 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "02" :orbit-number 5 :pcs-time 0 :si-vis-utilization 163 :al-overhead-at-end 0 :internal-dur-at-end 699 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) true 5 4 The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. 1642789376065 5714 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/royle/OP-cache/16793-v03.xml Epoch 10 of 13 is a 4-orbit (pseudo)CVZ visit, using the opportunity at ORIENT = 300 degrees. After guide star acquisition at the start of the first orbit, the guide star remains visible and locked for the duration of the visit, so no guide star re-acquisition in subsequent orbits will be required in orbits 2--4. This strategy is the same as adopted for GO-15278 in Cycle 25, and as successfully executed through Cycle 28. Specified POS_TARGs with respect to the nominal field center place the instrument apertures at the intended location within the 13-epoch pattern. While APT throws an error for the specified Bright Earth Avoidance angle of 13.5 degrees, this value is intended, and proven to schedule and execute successfully for a pseudo-CVZ visit. 1643661855000 302.8 (Tic-Visit :proposal-id 16793 :visit-id "03" :proposal-version -1 :trans-version "20210514" :date "21-Jan-2022 13:22:55.0" :trans-errors '(:WARNINGS 21 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 13.5 :data-volume 7430512 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16793 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16793 :visit-id "03" :orbit-number 1 :pcs-time 383 :si-vis-utilization 5332 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "03" :orbit-number 2 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "03" :orbit-number 3 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "03" :orbit-number 4 :pcs-time 0 :si-vis-utilization 5698 :al-overhead-at-end 0 :internal-dur-at-end 17 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "03" :orbit-number 5 :pcs-time 0 :si-vis-utilization 0 :al-overhead-at-end 0 :internal-dur-at-end 682 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) true 5 3 The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. 1633379874638 5714 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. Epoch 11 of 13 is a 4-orbit (pseudo)CVZ visit, using the opportunity at ORIENT = 244 degrees. After guide star acquisition at the start of the first orbit, the guide star remains visible and locked for the duration of the visit, so no guide star re-acquisition in subsequent orbits will be required in orbits 2--4. This strategy is the same as adopted for GO-15278 in Cycle 25, and as successfully executed through Cycle 28. Specified POS_TARGs with respect to the nominal field center place the instrument apertures at the intended location within the 13-epoch pattern. While APT throws an error for the specified Bright Earth Avoidance angle of 13.5 degrees, this value is intended, and proven to schedule and execute successfully for a pseudo-CVZ visit. 1648151632000 244.0 (Tic-Visit :proposal-id 16793 :visit-id "04" :proposal-version -1 :trans-version "20210514" :date "04-Oct-2021 13:37:52.0" :trans-errors '(:WARNINGS 23 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 13.5 :data-volume 6857536 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16793 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16793 :visit-id "04" :orbit-number 1 :pcs-time 383 :si-vis-utilization 5332 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "04" :orbit-number 2 :pcs-time 0 :si-vis-utilization 5695.0 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "04" :orbit-number 3 :pcs-time 0 :si-vis-utilization 5695.0 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "04" :orbit-number 4 :pcs-time 0 :si-vis-utilization 4680.0 :al-overhead-at-end 0 :internal-dur-at-end 1015.0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) true 4 3 The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. 1652209867332 5714 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/royle/OP-cache/16793-v05.xml Epoch 12 of 13 is a 4-orbit (pseudo)CVZ visit, using the opportunity at ORIENT = 191 degrees. After guide star acquisition at the start of the first orbit, the guide star remains visible and locked for the duration of the visit, so no guide star re-acquisition in subsequent orbits will be required in orbits 2--4. This strategy is the same as adopted for GO-15278 in Cycle 25, and as successfully executed through Cycle 28. Specified POS_TARGs with respect to the nominal field center place the instrument apertures at the intended location within the 13-epoch pattern. While APT throws an error for the specified Bright Earth Avoidance angle of 13.5 degrees, this value is intended, and proven to schedule and execute successfully for a pseudo-CVZ visit. 1652879005000 198.0 (Tic-Visit :proposal-id 16793 :visit-id "05" :proposal-version -1 :trans-version "20211222" :date "10-May-2022 15:11:06.0" :trans-errors '(:WARNINGS 22 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 13.5 :data-volume 7430512 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16793 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16793 :visit-id "05" :orbit-number 1 :pcs-time 383 :si-vis-utilization 5332 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "05" :orbit-number 2 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "05" :orbit-number 3 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "05" :orbit-number 4 :pcs-time 0 :si-vis-utilization 5567 :al-overhead-at-end 0 :internal-dur-at-end 148 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "05" :orbit-number 5 :pcs-time 0 :si-vis-utilization 0 :al-overhead-at-end 0 :internal-dur-at-end 551 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) false 5 3 The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=10. APT has no knowledge of this raised natural background, hence issues a warning. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=10. APT has no knowledge of this raised natural background, hence issues a warning. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=10. APT has no knowledge of this raised natural background, hence issues a warning. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=9. APT has no knowledge of this raised natural background, hence issues a warning. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=9. APT has no knowledge of this raised natural background, hence issues a warning. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=9. APT has no knowledge of this raised natural background, hence issues a warning. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=9. APT has no knowledge of this raised natural background, hence issues a warning. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=12. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, this requirement becomes satisfied for FLASH=12. 1656600564489 5714 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. /private/var/folders/8t/mg1bkfyj20xf2vfc_9vyhfs80006z1/T/OPVisit8864375551046301249.xml Epoch 13 of 13 is a 4-orbit (pseudo)CVZ visit, using the opportunity at ORIENT = 147 degrees. After guide star acquisition at the start of the first orbit, the guide star remains visible and locked for the duration of the visit, so no guide star re-acquisition in subsequent orbits will be required in orbits 2--4. This strategy is the same as adopted for GO-15278 in Cycle 25, and as successfully executed through Cycle 28. Specified POS_TARGs with respect to the nominal field center place the instrument apertures at the intended location within the 13-epoch pattern. While APT throws an error for the specified Bright Earth Avoidance angle of 13.5 degrees, this value is intended, and proven to schedule and execute successfully for a pseudo-CVZ visit. (Tic-Visit :proposal-id 16793 :visit-id "06" :proposal-version -1 :trans-version "20220516" :date "30-Jun-2022 10:49:24.0" :trans-errors '(:WARNINGS 23 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 13.5 :data-volume 7430512 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16793 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16793 :visit-id "06" :orbit-number 1 :pcs-time 383 :si-vis-utilization 5332 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "06" :orbit-number 2 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "06" :orbit-number 3 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "06" :orbit-number 4 :pcs-time 0 :si-vis-utilization 5715 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16793 :visit-id "06" :orbit-number 5 :pcs-time 0 :si-vis-utilization 32 :al-overhead-at-end 0 :internal-dur-at-end 699 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5714.0 :pcs-gap 0 ) true 5 4 The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=11. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=10. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high. The specified POS_TARG values intentionally place the WFC3/UVIS and ACS/WFC instrument apertures off the coordinates of the target (i.e., the center of the JWST NEP Time-Domain Field) to their intended locations within an annulus surrounding the extant HST data. Following the June 4 2020 recommendations of J. Anderson (2020) "CURRENT CTE-MITIGATION RECOMMENDATIONS", we aim for a minimum background level of 20 e-/pix in each WFC3/UVIS F275W exposure. Taking into account the raised natural background of this pseudo-CVZ visit, the WFC3/UVIS ETC shows that this requirement becomes satisfied for FLASH=12. The APT Phase-II diagnostics seem to still test the older (now superseded) recommendation of a minimum of only 12 e-/pix, and therefore result in a warning that the specified postflash may be too high.